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V773 Tau: a compact quintuple Pre-Main Sequence system?

Keck Science Meeting − October 15, 2010. Gaspard Duchêne (UC Berkeley, Obs. Grenoble) Andy Boden (Caltech) , Guillermo Torres ( CfA Harvard) , Andrea Ghez (UCLA) , Quinn Konopacky (LLNL). V773 Tau: a compact quintuple Pre-Main Sequence system?. High-order multiple systems.

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V773 Tau: a compact quintuple Pre-Main Sequence system?

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  1. Keck Science Meeting − October 15, 2010 Gaspard Duchêne (UC Berkeley, Obs. Grenoble) Andy Boden(Caltech), Guillermo Torres (CfA Harvard), Andrea Ghez(UCLA), Quinn Konopacky(LLNL) V773 Tau: a compact quintuple Pre-Main Sequence system?

  2. High-order multiple systems • Rare, but present in the field (up to N=7) • Mizar, Castor, ADS 9731, νSco • Formation in multiple phase • Two levels of fragmentation • Dynamical interactions (tides, scattering, exchange) • No known system above N=5 in PMS phase • But surveys are largely incomplete… • Are they formed and stable by the PMS stage? Keck Science Meeting – October 15, 2010 – Berkeley

  3. V773 Tau: a PMS quadruple • One of the brightest PMS star in Taurus • M★ ~ 1.5 M, age 3−5 Myr (from HR diagram) White & Ghez (2001) DSS R 2MASS K IRAC 4 V773 Tau 5000 AU Keck Science Meeting – October 15, 2010 – Berkeley

  4. V773 Tau: a PMS quadruple • One of the brightest PMS star in Taurus • M★ ~ 1.5 M, age 3−5 Myr (from HR diagram) • A complex quadruple system • A: SB2 (P = 51d) , q ~ 0.75 • B: unknown SpT(early-M?) Duchêne et al. (2003) NIRC2 A B C 25 AU V773 Tau A Welty (1995) Keck Science Meeting – October 15, 2010 – Berkeley

  5. A-B orbit: first estimate A B C • Based on 12 yr of astrometric monitoring • P ~ 46 yr • a ~ 20 AU • MAB ~ 3.7 ± 0.7 M [ D = 148pc ] • MB ~ 0.7 M • Linear motion for C • a ≥ 115 AU NIRC + NIRSPAO + NIRC2 1990 B A 2002 C Duchêne et al. (2003) Keck Science Meeting – October 15, 2010 – Berkeley

  6. Aa-Ab orbit: 3D modeling A B C Keck Interferometer • Integrated modeling of the KI V2, VLBI separations and RV monitoring • M(Aa) = 1.54 ± 0.14 M • M(Ab) = 1.33 ± 0.10 M • D = 136.2 ± 3.7 pc • Indirect estimate for B : • M(B) ~ 0.1 M (?) 4 mas ~ 0.5 AU Boden et al. (2007) Keck Science Meeting – October 15, 2010 – Berkeley

  7. A-B orbit: cont’d monitoring A B C • Goal: improve on dynamical mass of B • V773 Tau B not seen at expected location! • Almost lost in speckle cloud (2-3 mag fainter) VLT NaCo NIRC2 NIRC2 0.2” Oct 2008 Sep 2009 Dec 2006 Boden et al. (in prep.) Keck Science Meeting – October 15, 2010 – Berkeley

  8. A-B orbit: cont’d monitoring A B C • Goal: improve on dynamical mass of B • V773 Tau B not seen at expected location! • Almost lost in speckle cloud (2-3 mag fainter) • Separation is less than half the expected value! VLT NaCo NIRC2 NIRC2 0.2” Oct 2008 Sep 2009 Dec 2006 Boden et al. (in prep.) Keck Science Meeting – October 15, 2010 – Berkeley

  9. A-B pair: updated orbit A B C • Much better orbital phase coverage • Radial velocity variations of the A barycenter  Fully constrained 3D Keplerian model Boden et al. (in prep.) Keck Science Meeting – October 15, 2010 – Berkeley

  10. A-B pair: updated orbit A B C • Orbital parameters changed dramatically: • Porb ~ 26 yr(instead of 46 yr), 75% covered • With updated VLBA distance (Loinard et al.), new estimate for M(B) ~ 2.2 ± 0.6 M • How can B be more massive than Aa, yet less luminous (1.5 Lvs 2.2 L)? • Is B an unresolved binary as well? Keck Science Meeting – October 15, 2010 – Berkeley

  11. B component: spectroscopy A B C • Goal: constrain the nature of B and estimate RV • SpT (B): K2-K5, very similar to A component NIRSPAO A Dec 2003 B Boden et al. (in prep.) Keck Science Meeting – October 15, 2010 – Berkeley

  12. B component: spectroscopy A B C • Goal: constrain the nature of B and estimate RV • SpT (B): K2-K5, very similar to A component • Line profile suggests B is an SB2! • Supports the picture of B being a q > 0.75 binary V773 Tau A V773 Tau B Boden et al. (in prep.) NIRSPAO Keck Science Meeting – October 15, 2010 – Berkeley

  13. Putting it all together • V773 Tau likely contains 5 stars within 300 AU ! • One of the most compact such system to date • The structure and long-term stability of the dusty environment of B is a fascinating topic V773 Tau B apoastron: ~0.5 AU (?) V773 Tau A apoastron: 0.5 AU V773 Tau AB periastron: 14 AU V773 Tau C Separation ≤ 300 AU Keck Science Meeting – October 15, 2010 – Berkeley

  14. Putting it all together • V773 Tau likely contains 5 stars within 300 AU ! • One of the most compact such system to date • The structure and long-term stability of the dustyenvironment of B is a fascinating topic • Actually, V773 Tau could bea sextuple system ! • A faint T Tauri star some 3200 AU away… Keck Science Meeting – October 15, 2010 – Berkeley

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